166 Fretp Museum oF NATURAL History — GEOLOGY, VOL. III. 
and rounded. They are either convex or concave. The convex sur- 
faces are of comparatively uniform slope, the concave, irregular and 
showing depressions resembling pittings, though these are rarely as 
well-defined as is usual in meteorites. Five of these pits which occur 
together in one concavity are approximately circular in outline, 
shallow, and have a diameter of about one centimeter each. On 
another portion of the stone two similar but smaller pits may be 
seen and on another portion a larger, crescent-shaped pit. Nothing 
in the shape or markings of the stone indicates orientation during 
flight. The general shape of the stone is, as already noted, irregular 
and the crust remarkably uniform in appearance. In color the crust 
is dull black with occasionally an inclination to a reddish shade. 
Seen under the lens it presents a porous, slaggy appearance with no 
indications of flow. The indications are that the surface fused in 
place. The pores of the slag are very minute and the crust strongly 
adherent. Grains of nickel-iron rounded by fusion can be seen here 
and there and occasionally spots from one to three millimeters in 
diameter having smoother crust appear. These doubtless indicate 
portions which for some reason fused somewhat more readily. The 
color of the interior of the stone is in general brownish-black resem- 
bling the black chondrites. A marked feature (shown in Fig. 2, 
Plate LV.) is that of large spots of a much lighter color scattered over 
the dark ground. These are best seen on polished sections. The 
color of these spots is a light gray, and so much lighter than the mass 
of the meteorite as to be very prominent. The spots vary in size, the 
largest seen covering nearly one square inch of surface. The outline of 
the spots 1s irregular but not strongly so, and tends to be curved rather 
than straight. There seems to be no indication megascopically of any 
separation other than that of color, of the substance of these spots 
from the remainder of the mass. The section in which they are best 
exhibited and that illustrated in Fig. 2, Plate LV, was made near 
one end of the meteorite. On a section parallel to this made about 
one centimeter nearer the interior, the larger spots while retaining 
their relative position were found to be much smaller, less than half 
the size of those on the outer section. They do not, therefore, extend 
uniformly through the meteorite. As solid bodies their shape is 
probably somewhat lens-like or flat-pyramidal. One spot which 
was small on the outer section was about twice as large on the inner 
section. Hence the spots are probably to be found scattered irregu- 
larly through the meteorite. The structure of the meteorite on the 
whole in respect to these spots is the same as that designated by Bre- 
